Containing over ∼1057∼1057 baryons, neutron stars (NSs) are gigantic nuclei rich in neutrons. With masses on the order of solar mass 𝑀⊙≈1.99×1030M⊙≈1.99×1030 kg and radii around 10 km, neutron stars are compact objects of extreme densities. Their compactness 𝐶=𝐺𝑀/𝑅...
9.1 The structure of neutron stars Neutron stars probably consist of a massive dense core surrounded by a thin crust with a mass ≲0.01M⊙ and a thickness of ≲1km [550]. The interface between crust and core occurs at the density ≈ρ/2, where ρ0=2.8×1014g cm−3 is the densi...
Neutron stars are highly dense remnants of massive stars that have collapsed, composed mainly of neutrons and other elementary particles. They are observable due to their strong magnetism, rapid rotation, and emission of radio radiation in a narrow cone. ...
1 INTRODUCTIONSystems of interacting fermions are in superuid phases at low enough temperatures. Thus the core and inner crust regionsof neutron stars consist mainly of superuid neutrons. The neutron superuid in the core, carrying the bulk of the mass andmoment of inertia of the star, is the...
The supernovae were described immediately thereafter, in relation to the latest discovery of the neutron stars, as " the transitions from ordinary stars into neutron stars, which in their final stages consist of extremely closely packed neutrons" [2] Theoretically, however, neutron stars were ...
the pulse duration of the gamma-driven neutrons is much shorter52,53due to the relativistic feature of the electron beam generatingγ-rays. Nowadays, the high-yield laser-drivenγand neutron-beam production schemes are based on applications of high-intensity multi-petawatt-class laser systems, wher...
of the lightest elements - lithium, helium and beryllium - completely contradict this conception." These isotopes consist of a compact nuclear core and a cloud made of diluted nuclear material - called 'heiligenschein' or 'halo'. A halo consists mostly of neutrons that are very weakly bound ...
Although n − n transition is suppressed for neutrons bound in nuclei by nuclear forces, it can be effective in neutron stars (NS) where the neutrons are bound by grav- ity. The transformation of neutrons into mirror neutrons should decrease the degeneracy pressure, thereby softening the ...
It should be stressed that the estimated tempera- ture within this simple approximation only accounts for contributions of the ideal gas of neutrons and protons (mass differences have been neglected). Especially at the low-density regions of the outer crust of the hybrid star (which is composed ...
For example, for pure neutrons the deviation is below 0.9% and for a strongly bound nucleus such as iron the deviation of the average mass from mu would only be ≈ 0.2%. Therefore, we use in the following m0 ≈ mu. We further use from now on the convention that all energies are ...